The Kepler Science Data Processing Pipeline has been described by [1]} and [2]}. The Pipeline architecture [3]} and framework [4]}, [5]} have also been documented. The source files associated with the final revision (SOC 9.3) of the Pipeline code base have been released to the community.http://github.com/nasa/kepler-pipeline A block diagram of the Pipeline is shown in Fig. REF . Pixel level calibrations are performed in the Calibration (CAL) component [6]}, [7]}, [8]}; late in the mission, a time-dependent two-dimensional bias correction was included with a new module named Dynablack [9]}, [10]}. Light curves are extracted by Simple Aperture Photometry (SAP) in the Photometric Analysis (PA) component [11]}, [12]} from pixels associated with each Kepler target star; the target photocenter (i.e., centroid position) is also computed for each target and cadence. Photometric apertures employed in PA were initially determined in the Target and Aperture Definitions (TAD) software component [13]}, [14]}; the primary consideration in defining the TAD photometric apertures was maximization of photometric signal-to-noise ratio (S/N). For the final Q1–Q17 Pipeline processing (DR25) with the SOC 9.3 code base, photometric apertures were determined in PA proper primarily to optimize photometric precision by minimization of CDPP [15]}, [16]}.
